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宽线区在活动星系核（Active Galactic Nucleus；简称AGN）的研究中扮演着重要角色。
其发射线轮廓反映宽线区动力学信息，从发射线还可以推断宽线区的温度，氢原子数密度等状态信息。
通过对连续谱和发射线光变的反响映射（Reverberation Mapping；简称RM）观测可以探究宽线区的
结构和动力学特征以及测量黑洞质量。因此近年来，反响映射逐渐成为AGN领域的研究热点。
% 宽线区产生的宽发射线携带非常多的信息，因此对宽发射线的监测分析一直是AGN相关领域中的热点。
但是经过多年观测，宽线区
的结构和动力学等仍然有待进一步探明。一系列的问题摆在我们面前，如宽线区起源于哪里，
是来自吸积盘还是来自尘埃环？宽线区的结构是几何薄还是几何厚的，和吸积盘、尘埃环之间的关系怎样？
高吸积率的吸积盘存在自遮挡效应，是否会导致宽线区分层？根据超爱丁顿吸积超大质量黑洞
（Super-Eddington Accreting Massive Black Hole；简称SEAMBH）的观测结果，宽线区的尺度和
吸积率之间存在相关，这种相关是否由自遮挡效应导致？

由于宽线区结构在秒差距（Parsec；缩写pc；约3.26光年）尺度以下，无法进行直接的空间分解，
对宽线区的几何和动力学研究主要通过反响映射方法进行。如上文所述，我们在 SEAMBH 的反响映射系列
观测研究中发现了时间延迟随吸积率变短，偏离\rl 关系的现象。本文通过一批新的 SEAMBH 目标的
反响映射测量结果，进一步验证了上述结论。

其中 \pgone 作为第一个被证认的类星体，其光谱和 SEAMBH 目标的典型光谱特征一致，我们也
对其进行了光谱监测。
\pgone 几乎拥有AGN的所有奇特性质，如从射电到$\gamma$射线全
波段的明显辐射和光变，射电到硬X射线均可见的喷流特征，小尺度喷流中还存在视超光速现象。\pgone 在
一些波段表现出 blazar 的快速光变特征，但是光谱能量分布(Spectral Energy Distribution；简称SED)
中还可以看到明显的大蓝包和发射线。这些复杂特征使 \pgone 在不同研究方向都成为典型代表，
多年来一直是类星体研究的热点目标。

尽管对 \pgone 的研究非常多，但是大部分研究都集中在其多波段性质和喷流等方向。关于\pgone 的宽线区，
人们还所知甚少。最重要的，由于没有可靠的方法估计黑洞质量，\pgone 的中心黑洞质量依然存在很大争议。
以上这些都亟待回答。
本文使用长达10年的光谱监测数据，对 \pgone 进行了一次高质量的反响映射测量。给出了 \pgone 
不同发射线相对于连续谱的时间延迟，并由此估计了 \pgone 中心黑洞质量。结合紫外\lya 发射线，Balmer
发射线和\feii 发射线的时间延迟，估计了不同发射线在宽线区的分布。通过 \hbeta 发射线速度
分解的时间延迟测量结果，估计了宽线区的结构特征。上述结果很好地回答了以上问题。

文章内容组织如下：

第一章介绍了活动星系核的主要性质，包括活动星系核的观测特征，分类，基本结构模型等。之后介绍了反响
映射测量的原理，数据分析中常用的方法等。最后讲述了 \pgone\ SED的主要特征，各波段的观测
性质，以及历史上的研究发现等。

第二章简单讲述了SEAMBH项目中测光和光谱从观测到数据处理的主要流程，对其中可能出现的问题进行了
简要归纳。

第三章展示了2015--2017年间SEAMBH反响映射观测的10个目标的测量结果。其中4个是重复观测，重复
测量的结果和 2013 年至 2015 年期间的观测结果一致。6个新目标具有更高的5100\AA 光度，对应的
时间延迟同样偏离 \rl 关系。

第四章我们使用将近10年的 \pgone 密集采样数据，完成了一次对其的反响映射测量，得到静止波长下 \hbeta,
\hgamma, \feii 相对 5100\AA 连续谱的时间延迟分别是$146.8_{-12.1}^{+8.3}$，
$146.5_{-9.7}^{+8.8}$，$322.0_{-57.9}^{+55.5}$天，采用维里化因子$f_{\rm BLR}=1.3$，计算
得到 \pgone 的黑洞质量是 $\bhm = (4.1_{-0.4}^{+0.3}) \times 10^8 M_{\odot}$。我们对还
\hbeta 发射线进行了速度分解的时间延迟测量，得到了较为复杂的速度分解时间延迟结构，大致和一个盘
结构的宽线区预期一致。考虑紫外发射线的时间延迟，我们发现 \pgone 的宽线区满足壳层结构模型，
其中高电离发射线位于宽线区内区，低电离发射线位于宽线区外区。我们还用{\tt GALFIT}软件对\pgone 的
哈勃望远镜图像（Huble Space Telescope；简称$HST$）进行分解，测量得到寄主星系的核球质量
为$M_* = 10^{11.3\pm0.7} M_\odot$。

\keywords{活动星系核，宽线区，反响映射，黑洞质量, 宽线区结构和动力学}% 中文关键词
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Broad Line Regions (BLRs) play an import role in studies of Active Galactic 
Nuclei (AGNs), as the emission lines from BLRs carry fruitful information. For example, emission line
profiles reflect BLR dynamics and temperature and gas density information.
Through reverberation mapping (RM) observations,
we can explore geometry and dynamics of BLRs, and measure black hole mass.
RM has been a hot topic in AGN research over the last decades. However, after many years' studies,
geometry and dynamics of BLRs still need to be further explored.
A series of issues remain to be answered, among which include 1) the origin of BLRs and
2) the connection between BLRs and torus. For Super-Eddington Accreting Massive Black
Holes (SEAMBHs), some studies show that the \hbeta\ lag
shortens with increasing accretion rate, which is predicted by the
self-shadowing effects of slim accretion disks. However, more
observations are still needed to conform this result.

As the first identified quasar, \pgone\ shows most of AGN observational characteristics. It has obvious radiation and flux variation in all band. 
A large scale jet was observed from radio to hard X-ray band.
The very long baseline interferometry (VLBI) observation find a small 
scale jet with superluminal motion. \pgone\ displays both 
the blazar-like (the jet with superluminal motion, rapid and strong 
variability) and Seyfert-like (the strong blue bump and the significant 
emission lines) features, which make \pgone\ a typical target in a series of 
AGN classifications.

Most of the research on \pgone\ focus on its multi-band properties and the jets. Little is known about the BLR.
More importantly, the BH mass of \pgone\ is still controversial 
because there is no reliable estimation.
Here we report a new RM campaign of \pgone\ with 10-year high-quality monitoring data to answer the doubt. In this thesis, we obtained the 
time lags of \hbeta, \hgamma, \feii, and 
estimated the mass of the BH by using the \hbeta\ time lag. combined with 
the UV line, we found that the 
emission lines are consistent with a stratified structure. We also got some 
dynamical information of the BLR from the velocity-resolved time lag 
measurements.

This thesis is organized as follows:

In Chapter one, we introduce main properties of AGNs, including the
observational characteristics, classifications, and the AGN unification model.
The principle of RM and the related methods in RM data analysis are then described.
Finally, we introduce the basic properties about \pgone.

In Chapter two, we briefly describe the data reduction of photometry and spectroscopy
for our SEAMBH observations and then summarize possible problems in
our SEAMBH observations.

In Chapter three, we present observational results of 10 SEAMBH targets during 2015-2017 campaign.
Among those 10 SEAMBHs, four targets were also monitored during 2013-2015 campaign.
The obtained results are in good agreement between the two campaigns and confirm the shortening of \hbeta\
lags for SEAMBHs. Six new targets have higher 5100\AA\ luminosities compared with the targets in
previous SEAMBH campaigns (2012-2015)
The \hbeta\ time lags of those six new targets also deviate from the \rl\ relation.


In Chapter 4, we use the spectroscopic data of \pgone\ as long as nearly 10 years to complete
new RM monitoring. The time lags of \hbeta, \hgamma, \feii\ relative to 5100\AA\
continuum are $146.8_{-12.1}^{+8.3}$，
$146.5_{-9.7}^{+8.8}$，$322.0_{-57.9}^{+55.5}$ days, respectively. By adopting a
virial factor of $f_{\rm BLR}=1.3$ and the time lag of \hbeta\, the black hole
(BH) mass of \pgone\ is $\bhm = (4.1_{-0.4}^{+0.3}) \times 10^8 M_{\odot}$.
We also measured the velocity-resolved time lags of the \hbeta\ emission
line, and concluded that the \pgone\ broad-line region may be a
rotation-dominated disk with some inflows. Along with the UV lines, we find that the BLR of 3C 273 has a
stratified structure, with higher-ionization
lines arising from inner regions and lower-ionization
lines from the outer part. From decomposition of the $HST$ images of \pgone, we obtain a
host stellar mass of $M_* = 10^{11.3\pm0.7} M_\odot$. 

\KEYWORDS{Active galactic nuclei, Broad line region, Reverberation mapping, 
Black hole mass, Super-Eddington, The geometry and kinetics of the BLR}% 英文关键词
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